Galaxies Across Cosmic Time Overview: 1. Epoch of Reionization (z>6) 2. Stellar Mass Functions to z~6 3. Deep Spectroscopy at z~2-3 4. Circumgalactic Medium (z<1) 5. AGN outflows
Unprecedented Galaxy Samples at z>=4 (from HST s blank fields only: CANDELS+HUDF) log Numbers 3.5 3 2.5 2 1.5 1 0.5 0 6000 (z~4) 3000 (z~5) 900 (z~6) 10500 z~4-10 galaxies (Bouwens+15, with HST) 480 (z~7) 220 (z~8) 6 (z~10) 3 4 5 6 7 8 9 10 11 Redshift Almost 1000 galaxies in the epoch of reionization at z>6 Current frontier: z~9-10 2
The Evolution of the UV Luminosity Function to z~10 Bouwens et al. 2015, in prep bright (1600 Å luminosity) 7 mag baseline faint See also: e.g. Oesch+10a/12, Bouwens+10a,11,12; Bunker+10, Finkelstein+10/14, Wilkins+10/11, McLure+10/13, Yan+12, Bradley+12,... 3
SFRD Evolution at z>8 1 Oesch et al. 2015 Time [Gyr] 2 1.4 1 0.8 0.6 0.5 0.4 log SFR Density [M /yr/mpc 3 ] 1.5 2 2.5 3 3.5 4 > 0.7 M /yr HFF A2744 4 Clusters GOODS N/S + HUDF09/XDF CLASH SFR Density Evolution (1+z) 3.6 4.5 3 4 5 6 7 8 9 10 11 12 13 Redshift Current estimates seem to indicate that the cosmic SFRD evolves more rapidly at z>8 than at lower redshift! see also: Zheng+12, Coe+13, Bouwens+13/14, Ellis+13, McLure+13, Ishigaki+14 4
Stellar Mass Functions to z=7 Grazian et al. 2014 - CANDELS
Stellar Mass Function of Quiescent vs Star-forming Galaxies Tomczak et al. 2014 - ZFOURGE/CANDELS
Dwarf Galaxies @ 1<z<3 HST Frontier fields 900 Galaxies now (in 3 of 7 clusters) 2000 total expected 10 6 <M*<10 9 Msun!!!! 100x fainter than previous surveys 7
LF Evolution Φ [Mpc -3 Mag -1 ] 10-1 10-2 10-3 10-4 10-5 This work 1.0 < z <1.6 1.6 < z <2.2 2.2 < z <3.0 Oesch et al. 2010 (1.0 < z < 1.5) Oesch et al. 2010 (1.5 < z < 2.0) α -1.9-2.0-21.0-20.5-20.0-19.5-19.0 M * -22-20 -18-16 -14-12 M 1500 [AB] -1.3-1.4-1.5-1.6-1.7-1.8 Alavi et al. (2015, in prep) 8
HST IR Grism Surveys Various HST grism surveys (WISP, 3D-HST, AGHAST) using WFC3-IR camera to take slitless grism spectroscopy of deep fields. Detect continuum + strong emission lines at z~1-3, with R~50. (Relevant for future WFIRST grism surveys.)
Example images and spectra from 3D-HST survey ~250,000 extracted spectra; ~24,000 down to H=24 Momcheva et al 2015 (arxiv:1510:02106)
Deep Spectroscopic Surveys at z~2-3 With new multi-object NIR spectrographs on 10m telescopes (MOSFIRE, KMOS), can do deep spectroscopic surveys at moderate resolution at z~2-3. Obtain full suite of rest-frame optical lines that are studied at low-z: probe star formation, dust attenuation, metallicity, ionization parameter, AGN activity, electron density, shocks, kinematics, outflows, etc The MOSDEF survey: Total sample of ~1500 galaxies and ~150 AGN at 1.4 < z < 3.8 in the CANDELS fields Kriek et al. 2015 Kriek et al. 2015
Mass-Metallicity-SFR at z~2 Dust Attenuation at z~2 Sanders et al. 2015 Reddy et al. 2015 Galaxy Kinematics at z~2 AGN Diagnostics at z~2 Price et al. 2015 Coil et al. 2015
From Sirio Belli
From Sirio Belli
Galaxy Growth and Quenching Less focus on major mergers as primary driver of galaxy evolution Minor Mergers and Secular Evolution Inside-out galaxy growth Bulge formation precedes quenching Two modes / timescales for quenching
Born%of%Violence,%%Living%in%Turmoil Feedback:%return%of%ionizing% radiation,%kinetic%energy,%and% metals%to%the%ism,%cgm,%and% IGM%by%massive%stars%and%black% holes% Accretion:%An%acquisition%of%gas%by% the%galaxy%disk,%either%from% satellites,%mergers,%the%igm,%or%a% galactic%fountain%aka%recycling% Galaxy:%a%complex%system%in% which%baryons%cycle%through% many%physical%phases% CGM:%Circumgalactic%Medium%where%accreting%gas%meets% feedback%material%perhaps%extending%to%r vir% Slide by Jessica Werk 2
Observed(Properties(of(the(CGM:(The(HI(Gas ((((((=(stariforming( ((((((=(quiescent(( (((((((((((((=(nonidetections( Point(size( (column(density 50 100 150 COSIHalos( PI:(Jason(Tumlinson( 134(orbits(with(HST/COS( Max(N HI (=(10 19( Min(N HI (=(10 14.5( Line(saturation(! many(of(these(are( lower(limits NB:(Blank(space(=(no(data HI A(cool((10 4 (K)(medium(with(high(covering(fraction(of(N HI (>(10 15 (cm I2( (exists( around(nearly(every(l*(galaxy,(even$ellipticals,(to(150(kpc.( 9
Mass$of$the$CGM$ Werk+$2014:$ $M CGM $>$2$x$10 10 $M!" " Stocke+2013:$$ M CGM $>$10 10 $M!" " $ $$ $ The$CGM$is$a$major$reservoir$of$galac4c$baryons,$containing$at$least$as$many$as$the$ disk,$and$within$reach$of$closing$the$baryon$budget$around$l*$galaxies$(werk+14)$ 12$
Gas Inflow Onto Galaxies Have detected unambiguous gas inflow at z~1, using LRIS on Keck: Martin et al. 2012
Palomar Cosmic Web Imager Integral field spectrograph covering full optical spectrum. Now detecting IGM in emission using Ly-alpha near quasars at 1.5 < z < 4. Beginning to map filaments of cold gas between galaxies, watch gas accretion in action (velocity gradients along filaments). Martin et al. 2015 Upcoming Keck Cosmic Web Imager will probe low surface brightness IGM gas.
AGN Demographics and Fueling Host demographics don t argue for AGN quenching star formation, in that AGN are found in all types of galaxies - little dependence on stellar mass, found in roughly similar fraction of star-forming and quiescent galaxies (even bulge-less galaxies!). Major mergers probably most relevant for fueling quasars, not moderate-luminosity AGN. Weak correlations are seen between SFR and AGN activity. The big open question is whether AGN-driven feedback is important for quenching star formation
AGN Outflows Now at z~2 can study moderate-luminosity AGN-driven outflows using NIR multi-slit spectrographs and IFUs: incidence, kinematics, physical extent outflow narrow line Leung et al. in prep Find a high incidence of AGN-driven outflows that are galaxy wide, in typical star-forming galaxies.
Summary The multi-wavelength deep fields with HST imaging have led to big changes! probing epoch of reionization with UV LFs at z>6 stellar mass functions to z~6 dwarf galaxies at z~3 New ways of thinking about galaxy growth and quenching: inside-out galaxy growth, importance of minor mergers, secular evolution, bulge growth precedes star formation quenching, multiple quenching timescales. We are now studying full suite of rest-frame optical emission lines at z~2-3 in large, representative galaxy and AGN samples (>1000 sources). Studying AGN feedback in detail (incidence, kinematics, spatial extent) in both quasar and moderate-luminosity AGN samples, out to z~2-3.